Abstract
The calculations that will be discussed in this paper were undertaken to determine if plausible theoretical arguments could be found to indicate that planetary nebulae represent the stage in the evolution of a star immediately before it becomes a white dwarf. The model for the formation of a planetary nebula that will be described may also be applicable for more massive stars than have been studied. However, since it is known that some population-II stars become planetary nebulae and since there is evidence that evolved population-II stars are less massive than 1 M ⊙ (Christy, 1966; Hayashi et al.,1962; Faulkner, 1966; Faulkner and Iben, 1966; Schwarzschild and Härm, 1966) only stars whose masses are less than 1 M ⊙ have been studied.
Supported in part by the National Aeronautics and Space Administration (NsG-496).
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Rose, W.K. (1968). Pulsational Instability and the Origin of Planetary Nebulae. In: Osterbrock, D.E., O’Dell, C.R. (eds) Planetary Nebulae. International Astronomical Union / Union Astronomique Internationale, vol 34. Springer, Dordrecht. https://doi.org/10.1007/978-94-010-3473-9_58
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DOI: https://doi.org/10.1007/978-94-010-3473-9_58
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